An improved high-resolution solar reference spectrum for earth's atmosphere measurements in the ultraviolet, visible, and near infrared

By Kelly Chance, R. Kurucz. 2010

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Updated Smithsonian Astrophysical Observatory Ozone Monitoring Instrument (SAO OMI) formaldehyde retrieval (2015, methodology): “We use the high-resolution solar spectrum recently published by Chance and Kurucz (2010).”
Pale Orange Dots: The Impact of Organic Haze on the Habitability and Detectability of Earthlike Exoplanets (2016, methodology): “Our modern solar spectrum was modeled by Chance & Kurucz (2010), and our “Archean” Sun uses a modified spectrum based on the wavelength-dependent solar evolution correction from Claire et al. (2012) for 2.7 Ga.”
Filling-in of near-infrared solar lines by terrestrial fluorescence and other geophysical effects: simulations and space-based observations from SCIAMACHY and GOSAT (2012, unknown): “…simulated ﬁlling-in of the 866 nm Ca II solar line for a spectrally constant additive signal of 0.2 mW m − 2 sr − 1 nm − 1 , for several different spectral resolutions including the limit at the native 0.01 nm resolution of the Chance and Kurucz (2010) spectrum (denoted monochromatic in the ﬁgure).”
The Sun as a star: observations of white-light flares (2011, background): “ has a larger contribution of the upper photosphere (the Ca II line). Since, however, a multitude of lines are present all over the optical solar spectrum, we have looked at the modeled spectrum from Chance and Kurucz (2010), the observed spectrum by Thuillier et al. (2004) and the observed identiﬁe”